Friday, Dec 1. 9:14 AM: Deustua discusses future plans (we wait for people to finish making changes in travel plans) - Sahar Allam will be co-ordinator for SNAP Calibration Team's simulation efforts contact her for issues in the simulation code or required data, etc. - wants to attach names (to be leads) to a number of projects - project 0: feasibility and impact of color calibration total run SNAPSim as-is with no noise, no errors verify that cosmology in equals cosmology out present results at SNAP Collab meeting, Jan 18-20, 2007 - project 1: feasibility and impact of color calibration total uncertainties of 0.5%, 0.8%, 1%, 2% these are (in essence) systematic uncertainties in slope of flux calibration one can then start breaking down this overall error in flux calibration into errors in individual pieces (filters, detectors, etc.), and see how each type of error affects results there is a definite need to extend the filter = SpectralFunction class for Calibration purposes to be more flexible Mostek has knowledge in this area, but is busy at U Indiana Tucker has some experience in this area Stoughton has some knowledge of Java programming Richmond might be able to help - project 11 (a new task): design calibration pipeline (see also project 8) - project 2: detector characteristics much of this becomes active at the pixel level we will postpone pixel-level action for some time - project 3: spectrophotometry with IFU we don't deal with this in this group - project 4: filter errors some effect are at the pixel level bubbles in glass, dust, non-uniformities some are at higher level one can do simple approximations of angle-of-incidence effects by playing with filter transmission functions - project 5: flatfield variations at the so-simple-it's-not-interesting level, one can simple add random gaussian error to each measurement at interesting levels, need close-to-pixel level simulations Richmond has a possible model of focal plane maybe it can be adapted for framework purposes it will be necessary to add spectral functions for lamps, fibers, reflective material, etc. we must figure out how to fit lamplight into framework (doesn't come through telescope like starlight) - project 6: effect of thermal variations on photometric precision we are not sure at what level this is meant if as simple as "change in focal length", maybe not too hard if means "basic change in PSF", maybe still not too hard if includes tilting optics, or change in properties of focal plane instruments, this is could be very involved one could use HST experience to get some idea for likely effects and their sizes - project 7: effect of focal plane behavior on PSF and astrometric solutions this refers to static properties of focal plane, we think could also refer to effects due to refocusing - project 8: optimal cadence for calibration maintenance this won't happen for a while depends on the nature of the calibration pipeline - project 9: end-to-end simulation of optimal calibration strategy this depends on several other items above - project 10: the overall error budget we can _start_ to address little pieces in quantitative fashion - then brief discussion of the supporting projects the rocket project to calibrate stars in optical and IR has not been funded (twice, now) can we provide additional scientific justification? Bohlin will look at photometric uncertainties as a function of the chosen standard stars Mufson and Mostek continue their work on filters and LEDs at Indiana 11:03 AM break 11:16: Smith: IRTF observing - submitted proposal to observe HST and SDSS standards with IRTF imaging low-res spectroscopy (0.8-2.5 microns, R=250) high-res spectroscopy (0.8-2.5 microns, R=2000) high-res spectroscopy (2.4-2.5 microns, R=2500) given 4 nights in 2006B requested 4 nights in 2007A - 4 nights 2006B Tucker and Allam and Smith all observed 2 usable nights earthquake actually helped IRTF by un-sticking shutter - 13 Oct 2006 Imaging of 9 WDs and solar analogs spectroscopy of 2 WDs - 14 Oct 2006 spectroscopy of 3 WDs - the future plans requested 4 nights in 2007A will request nights in 2007B do we want to try HST proposal again? was rejected once before do we want to try Spitzer proposal again? not much time left TAC comments: you are picking the wrong IR standards should we try an HST proposal using NICMOS, forget Spitzer? probably ... use high-precision cosmology in general as justification Bohlin: what are the desired target stars? Bohlin: best standards are spectral type A next are type K (?) we want to pick some fainter stars which are in the SNAP fields (?) - the next collaboration meeting is Jan 18-20, 2007, in Berkeley French want to have a meeting to talk with Calib team on the day _before_ or _after_ the collab meeting to discuss their work on the spectrograph should that extra meeting be Wed, Jan 17? yes will the Calibration Team have anything to say? maybe, maybe not -- proabably not worth scheduling time - AAS meeting Jan 5-10, 2007, in Seattle, WA some people will be presenting posters